BEYOND THE NEXT GENERATION - (INO, T2HKK, ESSNSB, THEIA) - JOSH KLEIN, UNIVERSITY OF PENNSYLVANIA
←
→
Page content transcription
If your browser does not render page correctly, please read the page content below
Beyond the Next Generation
(INO, T2HKK, ESSnSB, THEIA)
Josh Klein, University of Pennsylvania 1
Where Will We Be?
“It’s hard to make predictions, especially about the future.” ---Yogi Berra
Probably:
• Mass ordering will be determined at several sigma
• Mixing matrix parameters all measured
•
• A supernova will have happened in the Milky Way
•
• Majorana phases unknown
• Understanding of neutrino interactions will be improved
Josh Klein, University of Pennsylvania 2
Where Will We Be?
“It’s hard to make predictions, especially about the future.” ---Yogi Berra
Probably:
• Mass ordering will be determined at several sigma
• Mixing matrix parameters all measured
• But not necessarily matrix elements independently
• A supernova will have happened in the Milky Way
•
• Majorana phases unknown
• Understanding of neutrino interactions will be improved
Josh Klein, University of Pennsylvania 3
Where Will We Be?
“It’s hard to make predictions, especially about the future.” ---Yogi Berra
Probably:
• Mass ordering will be determined at several sigma
• Mixing matrix parameters all measured
• But not necessarily matrix elements independently
• A supernova will have happened in the Milky Way
• But neutrinos may not have arrived yet
• Majorana phases unknown
• Understanding of neutrino interactions will be improved
Josh Klein, University of Pennsylvania 4
Where Will We Be?
“It’s hard to make predictions, especially about the future.” ---Yogi Berra
But…?
• Sterile evidence/discovery?
• Dm212 tension between reactor and solar?
• Majorana vs. Dirac?
• Absolute neutrino mass?
• A theory of flavor…?
• Other tensions/anomalies/problems…?
Josh Klein, University of Pennsylvania 5
Where Will We Be?
Goals for experiments beyond next generation:
• Precision tests of the 3-flavor model
• e.g., Is d maximal?
• e.g., Is leptonic CP described entirely by d?
• Focus on reduction of systematics
• Searches for new physics
• Investigating new (and possibly old) anomalies
• Astrophysical/geophysical measurements and precision tests
• Continued exploration of the Majorana question
• Continued work to measure absolute masses
Josh Klein, University of Pennsylvania 6
India-Based Neutrino Observatory (INO)
Goal: Precision tests of 3-flavor model with atmospherics
85-ton prototype, 4m´4m´11 layer magnet, with 2mx2m
RPCs and ICAL electronics operating for 2 years.
51 kt Magnetized Iron Calorimeter
Mini-Cal
Sample cosmic muon tracks
INO @ Theni, Tamil Nadu
Proposed 51 kton
magnetized Iron
CALorimeter (105m2 glass Comparison of azimuthal muon flux with Comparison of the muon momentum spectra
RPC, 3.6M CORSIKA and HONDA simulations with CORSIKA simulations, negative (positive) 7
values correspond to µ+(µ-)
electronics channels)
Engineering Toward Full ICAL INO
Size 4.6m×4.6m×1.8m, extruded plastic
Scintillator Veto for mini-ICAL
scintillators (courtesy Fermilab), muon
efficiency > 99.99% Scintillator veto
upgrade for Mini-CAL
700 ton
magnetised ICAL
prototype
(8m×8m× 2.1m,
with 352 RPCs,
45K electronics
channels)
Industrial production of RPC
detectors and closed loop gas
system for the engineering
prototype
INO
Physics Sensitivities
Combination of high
mass, tracking, and
charge ID via magnet,
provides precision
handle on atmospheric
direction and energy
up to 25 GeV
T2HKK/KNO
Goal: Precision measurements of PMNS parameters+broad program
Remarkable luck:
J-PARC beam re- KNO
Flower
emerges in Korean
Neutrino
Korea— Observatory
Hyper-
Kamiokande is the
“near detector” 1~3 deg. off-axis Tokai to(2) HK to Korea
~1000 m
km km km km km km
overburden
provides broad
program
Josh Klein, University of Pennsylvania 10T2HKK/KNO
Off-axis beam+long baseline---
Sensitivity to 2nd oscillation max 10 yrs
enhancing CPV sensitivity
Precision on dcp
True Normal Ordering True Inverted Ordering significantly
improved with
30 30
sd (°)
sd (°)
JD´1 JD´1
Bisul
cp
JD´2
cp
JD´2
25 JD+KD at 2.5°
25 JD+KD at 2.5°
20
JD+KD at 2.0°
JD+KD at 1.5° 20
JD+KD at 2.0°
JD+KD at 1.5° KNO---
15 15 Single HK has
sdcp~22o
10 10
5
Normal
5
Inverted
0
0 1 2 3 4 5 6
dcp (rad.)
0
0 1 2 3 4 5 6
dcp (rad.)
with KNO+HK
sdcp~13o
Additional matter allows
high sensitivity to MO At max CPV
(and sensitivity to NSI)
Prog. Theor. Exp. Phys. 2018, 063C01 11T2HKK/KNO
Broad program
beyond LBL
oscillations
SuperNova Relic n
p à e+ p0 p à n K+
• Additional mass and depth provide excellent NDK sensitivity
• Low photocoverage could be compensated by Gd loading
~100 events
(5s)
• KNO Organization and WGs formed in 2018
• Sensitivity studies and Detector R&D in progress
• Funding for KNO feasibility studies from Korean
government granted in May 2020
Josh Klein, University of Pennsylvania 12
Josh Klein, University of PennsylvaniaESSnSB nd
Goal: CPV via targeted measurements at 2 Oscillation Max
Neutrino Superbeam at Garpenberg
European Spallation Source Zinkgruvan (1200 m)
(1500 m) Also about 1020 µ/year
produced---provides
R&D opportunity for
Neutrino Factory or
muon collider
540 km
360 km
@ Far Site:
o Megaton-scale underground Water Cherenkov detector
Lund, Sweden Allows broad program including
PDK, astrophysical ns T. Tolba #66
o 5 MW/2.5 GeV protons
o accumulation ring of ~400 m
o Shortens pulse from 2.86 ms to few µs
o Required by 350 kA horn
o Also allows for decay-at-rest experiments using neutron target
o 4 target/horn system, 25 m decay tunnel
o ~300 MeV neutrinos
o near detector
Josh Klein, University of Pennsylvania 13ESSnSB
2nd Oscillation max provides excellent Physics Sensitivities
CP sensitivity
0.20
δ = - π/2
ν
> 5 s for 60% of CP phase space Far site may depend on
δ=0
0.15
NH δ = π/2 5% syst. (signal) prior results
IH 10% syst. (background)
P e
2nd Osc. Max
νμ→ν
L = 540 km
0.10 E= 2.5 GeV
At dcp=0 or p; 5o resolution
At max CP, as low as 12o
0.05
0.00
0.2 0.4 0.6 0.8 1.0
E [GeV]
Large detector size provides big
atmospheric sample for higher sensitivity,
resolution of q23 octant Josh Klein, University of Pennsylvania 14ESSnSB
Status and Progress
• ESSnuSB: H2020 Design Study, 4.7 M€ (3 M€ by EU)
• 17 institutes including ESS and CERN
• Approved in August 2017
• Started beginning of January 2018 2035-:
Data
• Duration: 4 years (2018-2021) 2027-2034: taking
2025-2026: Construction of
2022-2024: Preconstructi the facility and
on Phase, detectors,
2021: End of Preparatory International including
Phase, TDR commissioning.
2018: ESSνSB Agreement
Design Study, Muon option
beginning of CDR and
2016-2019: ESSνSB also possible.
beginning of Design preliminary
2012: COST costing
Action Study (EU-
inception of H2020)
the project EuroNuNetTHEIA
Goal: A very broad range of world-leading physics
keV MeV GeV TeV
KamLAND
Borexino
Solar ns Long Baseline Extragalatic ns
Geo, reactor n Atmospherics
DSNB
SN burst ns Requirements:
• Excellent PID
0nbb • Directional information
Super-Kamiokande
• Very big detector SNO
Requirements:
• Low radio backgrounds
SNO+
• Excellent energy resolution
• Directional informationJosh Klein, University of Pennsylvania 16THEIA
125
Attenuation length (m)
Hybrid Cherenkov/Scintillation Water-based liquid
Water (SK,SNO)
100 scintillator (WbLS)
75
scintillation
Water-based Liquid Scintillator
kov Water-like Oil-like
re n 50 § >70% water § loading of
h e § Cherenkov+ hydrophilic
C scintillation elements
§ cost-effective
25
Scintillator
Borexino
KamLAND
0
102 103 104
Photon yield (MeV)
Target can be adjusted for different physics goals
Josh Klein, University of Pennsylvania 17Many new
THEIA Multiple independent handles achieve:
Timing Spectrum Angular distribution • 90% purity for Chertons
technologies for “instantaneous chertons” UV/blue scintillation vs. increased PMT hit density • Little loss of scintons
discriminating vs. delayed “scintons”
→ ns resolution or better
blue/green Cherenkov
→ wavelength-sensitivity
under Cherenkov angle
→ sufficient granularity FlatDot Gruszko et
“chertons” from measurements al, JINST 14
(2019) 02,
“scintons” P02005
LAPPDs
LAB
M. Wurm
Spectral sorting--Dichroicons
Slow Fluors
CHESS
Chertons Measurements
Caravaca et al,
J. Paton #422 arXiv2002.00173(2020)
Scintons
Kaptanoglu et
5% WbLS
al, PRD 101 Caravaca et
(2020) 7, al, EPJC
r to n
Ch e
072002
to n s
L. Pickard #551 Biller, Leming, Paton NIMA 972 (2017) 77:811
scin
B. Land #472 18
(2020) 164106 LAB-PPO
J. Caravaca #490THEIA Long-baseline oscillations
G. Yang #253
Examined two detectors @ LBNF:
Assumes
THEIA-25 (kt) THEIA-100 (kt) • LBNF beam
• Super-K like performance
• Scintons ignored
• T2K-like reconstruction
(“fitQUN”)
• Includes multi-ring events
• Systematics like DUNE
CDR
• ”3DST” scintillator near
detector THEIA-25 (17 kt fid.) ~ Single DUNE 10 kt
THEIA-100 (70 kt fid) > 3 s CP sensitivity
over large fraction of phase space
Josh Klein, University of Pennsylvania 19
Phased program to increase light yield, Cher/Scint separationPrecision CNO
measurement via pointing
THEIA
Possibility of CC on 7Li for 8B and SN
n astrophysics
DSNB Background rejection
M. Smiley #312 MSW “Clean” geo-neutrino signal exploiting Cher/Scint Ratio
Transition
Region
THEIA-100 THEIA-100 Allows U/Th measurement
SN Burst neutrino spectra SN pointing ~ 2 degrees
Pre-SN burst neutrinos
10 kpc
D. Guffanti #475
THEIA-100
THEIA-100 Low reactor/geo background--
Burst Trigger latency ~100 ns
~200 events total from LMC 3 s detection 1 day before SN
IBD tagging via n capture out to 3.3 kpc
Literally complementary to LAr Josh Klein, University of Pennsylvania 20THEIA Beyond the Standard Model
Neutrinoless Double Beta Decay Nucleon Decay
Requires inner Dominant 8B n background
containment bag for reduced by pointing
high LY scintillator Size and scintillation light
M. Askins #543
provides excellent sensitivity
to “invisible modes”
Detection of K+ via
scintillation light
T1/2 > 1028 y in 10 y for Te loading
Assumes:
• 5% loading of natTe
• 3% energy resolution at endpoint
• 50% removal of 8B n background
See also talk by J. Detwiler and
21
S.D. Biller PRD 87 (2013) 7, 071301 Josh Klein, University of Pennsylvania?
Might make sense if scintillator adds to PID or background rejection at high energy
Or to broaden programs if depth accommodates it
But transparency of scintillator might limit size of detector
Josh Klein, University of Pennsylvania 22Summary
• Exciting prospects for future large-scale experiments!
• Broad suite of creative R&D driving capabilities
• A lot will depend on what the current generation tells us…
Thanks to INO, T2HKK, ESSnSB and THEIA Collaborations!
Josh Klein, University of Pennsylvania 23You can also read
